Exploring physical properties of minimally deformed strange star model and constraints on maximum mass limit in $f(\mathcal{Q})$ gravity

TL;DR

This paper models compact stellar objects using $f( ext{Q})$ gravity and the MGD technique, aiming to explain the GW190814 event's secondary component with new solutions influenced by key parameters.

Contribution

It introduces new classes of anisotropic star solutions in $f( ext{Q})$ gravity using MGD, linking parameters to stability and mass predictions relevant to GW190814.

Findings

Parameters $ ext{Q}$ and $eta$ influence stability and thermodynamics.

Models predict masses consistent with GW190814's secondary component.

New solutions depend on metric deformation and anisotropy.

Abstract

In this work we take our cue from the observations of gravitational waves of the GW190814 event which suggests that source of the signals can be ascribed to a compact binary coalescence of a 22.2 to 24.3$ M_{\odot}$ black hole and a compact object endowed with a mass of 2.50 to 2.67$M_{\odot}$. In the current exposition, we are concerned with modeling of the lower mass component of the coalescence pair. We utilise the $f(\mathcal{Q})$ gravity together with Minimum Geometric Deformation (MGD) technique to obtain compact stellar objects with masses aligned with the GW190814 event. Starting off with the Tolman IV ansatz for one of the metric functions, together with a MIT Bag model equation of state we are able to reduce the problem of fully describing the gravitational behaviour of the seed solution to a quadrature. Through the MGD technique, we introduce anisotropy by deforming the radial part of the gravitational potential. This enables us to obtain two new classes of solutions which depend on the metricity parameter, $\cal Q$ and the deformation constant, $\beta$. We show that these two parameters play a crucial role in determining the thermodynamical behaviour and stability of our models. In particular, we show that the interplay between the metricity parameter and the deformation constant leads to predicted mass of the progenitor articulating as the secondary component of GW190814.